Three-component modelling of C-rich AGB star winds – IV. Revised interpretation with improved numerical descriptions

摘要: Models describing dust-driven winds are important for understanding the physical mechanism and properties of mass loss on asymptotic giant branch. These models becoming increasingly realistic with more detailed physics included, but also computationally demanding. The purpose this study is to clarify what extent applied numerical approach affects resulting structures modelled winds, discuss changes. Following previously developed radiation hydrodynamic model - which includes descriptions time-dependent dust formation gas-dust drift using its assumptions parameters, improvements introduced. Impacts so-called adaptive grid equation advection schemes assessed from calculated different setups. Results show that wind strongly influenced by imprecision, displaying differences in up 100 per cent. Using a non-adaptive grid, become periodic (in multiples stellar pulsation periods), instead irregular, as obtained previously. Furthermore, reveal changes structures. influence confirmed be highly important, particular component. Gas less tightly coupled than previously, drastically larger amounts form assuming drift.